\documentclass{article}
\textwidth 18cm
\textheight 23cm
\oddsidemargin -1cm
\topmargin 0cm
\parskip 0.15cm
\parindent 0pt
\small
\begin{document}
\def\izq#1{\hbox to -1.5pt{\hss#1}}
\arrayrulewidth 0.04cm
%VERSION 3
\begin{center}
\begin{tabular}{|p{6.0cm}|p{8.5cm}|} \hline
& \\
\multicolumn{1}{|l|}{\hspace{0.5cm}\LARGE\bf\sf Active}
& \multicolumn{1}{|c|}{\large\em An electronic publication dedicated to}\\ [0.3cm]
\multicolumn{1}{|l|}{\hspace{0.5cm}\LARGE\bf\sf Galaxies} & \multicolumn{1}{|c|}{\large\em the observation and theory of}\\ [0.3cm]
\multicolumn{1}{|l|}{\hspace{0.5cm}\LARGE\bf\sf Newsletter} & \multicolumn{1}{|c|}{\large\em active galaxies}\\ [0.3cm]
\hline
& \\
\multicolumn{1}{|c|}{\large\bf\sf No. 86 --- May 2004 } &
\multicolumn{1}{|c|}{\bf\sf Editor: Rob Beswick (rb@ast.man.ac.uk)} \\ [-0.1cm]
& \\ \hline
\end{tabular}
\end{center}
\small
\begin{center}
{\Large\em Abstracts - Thesis Abstracts - Jobs - Meetings}
\end{center}
\begin{center}
{\Large\sf From the Editor}
\end{center}
\vspace*{0.6cm}
The Active Galaxies Newsletter is produced monthly. The deadline for
contributions is the last friday of the month. The Latex macros for
submitting abstracts and dissertation abstracts are appended to each
issue of the newsletter and are also available on the web page.
\begin{center} Rob Beswick \end{center}
\vspace*{1cm}
\begin{center}
{\Large\sf Abstracts of recently accepted papers}
\end{center}
\vspace*{0.6cm}
{\large\bf{Evidence for a multizone warm absorber in the {\it
XMM-Newton} spectrum of Markarian 304}}
{\bf{ E.~Piconcelli$^1$, E.~Jimenez-Bailon$^1$, M.~Guainazzi$^1$,
N.~Schartel$^1$, P.M.~Rodriguez-Pascual$^1$ \& Maria Santos-Lleo$^1$
}}
$^1$ {XMM-Newton Science Operation Center (ESA), Apartado 50727, E-28080
Madrid, Spain}
{We present a {\it XMM-Newton} observation of Markarian 304, a Seyfert 1
galaxy at $z$ = 0.066. The {\it EPIC} data show that MKN~304 is affected
by heavy (N$_{\rm H} \approx$ 10$^{23}$ cm$^{-2}$) obscuration due to
ionized gas. A two--phase warm absorber provides an adequate
parameterization of this gas. The ionization parameter of the two
components is $\xi \approx$ 6 erg cm$^{-2}$ s$^{-1}$ and $\xi \approx$
90 erg cm$^{-2}$ s$^{-1}$, respectively. The observed continuum photon
index ($\Gamma \approx$ 1.9) is typical for Seyfert 1 galaxies. Two
significant emission lines are detected at 0.57 keV and 6.4 keV,
respectively. The former is mostly likely due to He--like oxygen
triplet emission arising from an ionized plasma (maybe the warm absorber
itself). The latter is due to fluorescent emission of K--shell iron in a
low--ionization state (FeI--XV). The upper limit for the line width of
$\sigma_{K\alpha} http://www.eso.org/~rsiebenm/FTP/3CRisocam.pdf \newline
%% -> http://www.eso.org/~rsiebenm/FTP/3CRisocam.ps.gz}
http://www.eso.org/$\sim$rsiebenm/FTP/3CRisocam.pdf \newline
http://www.eso.org/$\sim$rsiebenm/FTP/3CRisocam.ps.gz}
\vspace*{0.3cm}
{\large\bf{XMM-Newton EPIC observations of 21 low-redshift PG quasars}}
{\bf{ D. Porquet$^1$, J.N. Reeves$^{2,3}$, P. O'Brien$^4$, W.
Brinkmann$^1$ }}
$^1$ {Max-Plank-Institut f\"{u}r extraterrestrische Physik, Postfach 1312,
D-85741, Garching, Germany} \\
$^2$ {Laboratory for High Energy Astrophysics,
NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA}\\
$^3$ {Universities Space Research Association}\\
$^4$ {Department of Physics and Astronomy,
University of Leicester, Leicester LE1 7RH, UK}
{We present an X-ray spectral analysis of 21 low redshift quasars
observed with {\sl XMM-Newton} EPIC. All the sources are Palomar Green
quasars with redshifts between 0.05 and 0.4 and have low Galactic
absorption along the line-of-sight. A large majority of quasars in the
sample (19/21) exhibit a significant soft excess below $\sim$
1--1.5\,keV, whilst two objects (PG\,1114+445 and I\,Zw1) show a deficit
of soft X-ray flux due to the presence of a strong warm absorber.
Indeed, contrary to previous studies with {\sl ASCA} and {\sl ROSAT}, we
find that the presence of absorption features near 0.6--1.0\,keV is
common in our sample. At least half of the objects appear to harbor a
warm absorber, as found previously in Seyfert 1 galaxies. We find
significant detections of Fe\,K$\alpha$ emission lines in at least
twelve objects, whilst there is evidence for some broadening of the line
profile, compared to the EPIC-pn resolution, in five of these quasars.
The determination of the nature of this broadening (e.g., Keplerian
motion, a blend of lines, relativistic effects) is not possible with the
present data and requires either higher S/N or higher resolution
spectra. In seven objects the line is located between 6.7--7\,keV,
corresponding to highly ionized iron, whereas in the other five objects
the line energy is consistent with 6.4 keV, i.e. corresponding to near
neutral iron. The ionized lines tend to be found in the quasars with the
steepest X-ray spectra. We also find a correlation between the continuum
power law index $\Gamma$ and the optical H$\beta$ width, in both the
soft and hard X-ray bands, whereby the steepest X-ray spectra are found
in objects with narrow H$\beta$ widths, which confirms previous {\sl
ROSAT} and {\sl ASCA} results. The soft and hard band X-ray photon
indices are also strongly correlated, i.e. the steepest soft X-ray
spectra correspond the steepest hard X-ray spectra. We propose that a
high accretion rate and a smaller black hole mass is likely to be the
physical driver responsible for these trends, with the steep spectrum
objects likely to have smaller black hole masses accreting near the
Eddington rate.}
{Accepted by Astronomy and Astrophysics }
{E-mail contact: dporquet@mpe.mpg.de, astro-ph/0404385}
\newpage
%\vspace*{0.6cm}
{\large\bf{ROSAT and ASCA observations of a narrow-line Seyfert 1 galaxy
RXJ0136.9-3510 : blueshifted Fe K$\alpha$ line Nan Nextended sof X- ray
emission}}
{\bf{ Kajal K. Ghoshi$^1$, Douglas A. Swartz$^1$, Allyn F. Tennant$^2$,
Kinwah Wu$^3$ \& Brian D. Ramsey$^3$ }}
$^1$ {USRA, NASA/MSFC/NSSTC SD 50, Huntsville, AL 35805.} \\
$^2$ {Space Science Department, NASA/MSFC/NSSTC, SD 50, Huntsville, AL
35805.} \\
$^3$ {MSSL, University College of London, Holmbury St. Mary, Surrey,
RH5 6NT, UK.}
{RX J0136.9-3510 is an unusual Narrow-line Seyfert 1 galaxy (NLS1). We
have detected extended ($\sim$12$^{\prime\prime}$ or $\sim$54 kpc at the
source frame) soft X-ray emission in the ROSAT HRI image, accounting for
20\% of the total emission. We have also detected a highly blueshifted
(7.6 keV in the source frame) Fe K$\alpha$ line in the ASCA SIS
spectrum. This is the first detection of such a highly blueshifted
emission line in a NLS1. Near-IR and FIR studies indicate the presence
of a possible starburst component in this NLS1. Physical models of the
accretion and/or outflow and the evolution of this NLS1 are discussed in
the context of these results. }
{Accepted by Astrophysical J. Lett. }
{E-mail contact: kajal.ghosh@msfc.nasa.gov}
\vspace*{0.6cm}
{\large\bf{Black Hole Masses from Reverberation Measurements}}
{\bf{ Bradley M. Peterson$^1$ }}
$^1$ {Department of Astronomy, The Ohio State University, 140 West 18th
Avenue, Columbus, OH 43210}
{We have reanalyzed in a consistent way existing reverberation data for
35 AGNs for the purpose of refining the black hole masses derived from
these data. We find that the precision (or random component of the
error) of reverberation-based black hole mass measurements is typically
around 30\%, comparable to the precision attained in measurement of
black hole masses in quiescent galaxies by gas or stellar dynamical
methods. As discussed in this volume by Onken et al., we have
established an absolute calibration for AGN reverberation-based masses
by assuming that AGNs and quiescent galaxies follow an identical
relationship between black hole mass and host-galaxy bulge velocity
dispersion. The scatter around this relationship implies that the
typical systematic uncertainties in reverberation-based black hole
masses are smaller than a factor of three. We present a preliminary
version of a mass--luminosity relationship that is much better defined
than any previous attempt. Scatter about the mass--luminosity
relationship for these AGNs appears to be real and could be correlated
with either Eddington ratio or source inclination.}
{To appear in The Interplay among Black Holes,
Stars and ISM in Galactic Nuclei,
ed. Th. Storchi Bergmann, L.C. Ho \& H.R. Schmitt }
{E-mail contact: peterson@astronomy.ohio-state.edu,\newline
preprint available at http://arxiv.org/abs/astro-ph/0404539}
\vspace*{0.6cm}
{\large\bf{High resolution observations of the neutral hydrogen
absorption and jets in 3C293}}
{\bf{R. J. Beswick,$^1$ A. B. Peck,$^2$ A. Pedlar,$^1$ G. B.
Taylor,$^3$ G. Giovannini,$^4$ J. P. Leahy$^1$ \& N. J. Jackson$^1$ }}
$^1$ Jodrell~Bank Observatory, The University of Manchester,
Macclesfield, Cheshire SK11~9DL, UK.\\
$^2$ Harvard-Smithsonian Center for Astrophysics, SAO/SMA Project,
P.O. Box\,824, Hilo, HI~9672, USA\\
$^3$ National Radio Astronomy Observatory, P.O. Box O, Socorro, NM
87801, USA\\
$^4$Istituto di Radioastronomia del CNR, via Gobetti\,101, 40129
Bologna, Italy
{We present results from new high angular resolution observations of the
neutral hydrogen absorption using global VLBI, MERLIN, \& VLA
observations of the peculiar radio galaxy 3C\,293. These results reveal
extensive H{\sc i} absorption against the inner kiloparsec of the radio
jet in this source over a wide range of angular scales. In additional to
these sub-arcsecond resolution radio observations we also present
infrared imaging of the jet.}
{To appear in The Interplay among Black Holes,
Stars and ISM in Galactic Nuclei,
ed. Th. Storchi Bergmann, L.C. Ho \& H.R. Schmitt }
{E-mail contact: rbeswick@jb.man.ac.uk,\newline
preprint available at
%% http://www.jb.man.ac.uk/~rbeswick/papers/papers.html
http://www.jb.man.ac.uk/$\sim$rbeswick/papers/papers.html}
\newpage
%\vspace*{0.6cm}
{\large\bf{A possible radio supernova in the outer part of NGC3310}}
{\bf{M. K. Argo$^1$, T. W. B. Muxlow$^1$, A. Pedlar$^1$, R. J.
Beswick$^1$ \& M. Strong$^1$}}
$^1$Jodrell Bank Observatory, The University of Manchester,
Macclesfield, Cheshire SK11~9DL, UK.
{As part of an on-going radio supernova monitoring program, we have
discovered a variable, compact steep spectrum radio source $\sim$65
arcsec ($\sim$4\,kpc) from the centre of the starburst galaxy NGC\,3310.
If the source is at the distance of NGC\,3310, then its 5\,GHz
luminosity is $\sim3 \times 10^{19}$\,W\,Hz$^{-1}$. The source
luminosity, together with its variability characteristics, compact
structure ($ \over \sim \;$}
\def\lsim{\lower.5ex\hbox{\ltsima}}
{Narrow-Line Seyfert 1 galaxies (NLS1s) and Narrow-Line quasars (NLQs)
seem to amount to $\sim 10-30 \%$ of active galactic nuclei (AGNs) in
the local universe. Together with their average accretion rate, we argue
that the black hole (BH) growth by factor of $8-800$ happens in these
super-Eddington accretion phase of AGNs. Moreover, there is a possible,
systematic underestimation of accretion rates (in the Eddington unit)
due to an overestimation of BH mass by massive accretion discs for
super-Eddington objects. If it is true, the factor of BH growth above
may be larger by order(s) of magnitude. In contrast, the growth factor
expected in sub-Eddington phase is only $\sim 2$. Therefore, the cosmic
BH growth by accretion is likely dominated by super-Eddington phase,
rather than sub-Eddington phase which is the majority among AGNs.
This analysis is based on the fraction and the average accretion rate of
NLS1s and NLQs obtained for $z \lsim 0.5$. If those numbers are larger
at higher redshift (where BHs were probably less grown), super-Eddington
accretion would be even more important in the context of cosmic BH
growth history.
}
{ Accepted for publication in Astronomy and Astrophysics Letters}
{E-mail contact: kawaguti@optik.mtk.nao.ac.jp,\newline preprint
available at http://arxiv.org/abs/astro-ph/0405024}
\begin{center}
\fboxrule0.02cm
\fboxsep0.4cm
\fbox{\rule[-0.9cm]{0.0cm}{1.8cm}{\parbox{14cm}
{
The Active Galaxies Newsletter is available on the World Wide Web.
You can access it via the University of Manchester home page :-
%%-> http://www.ast.man.ac.uk/~rb/agn/
http://www.ast.man.ac.uk/$\sim$rb/agn/
\newline
If you move or your e-mail address changes, please send the editor
your new address. If the Newsletter repeatedly bounces back from an
address then that address is deleted from the mailing list.
}}}
\end{center}
\end{document}
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
%%% %%%
%%% LaTeX macro for the Active Galaxies Newsletter %%%
%%% Please use the following macro for your recently accepted paper %%%
%%% and return to rb@ast.man.ac.uk %%%
%%% %%%
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
\documentstyle{article}
\textwidth 18cm
\textheight 23cm
\oddsidemargin -1cm
\topmargin 0cm
\parskip 0.15cm
\parindent 0pt
\small
\begin{document}
%\vspace*{0.6cm}
%% Between these brackets you write the title of your paper:
{\large\bf{Title of Paper}}
%% Here comes the author(s) of the paper, please indicate within $^...$
%% the number which corresponds to the institute of each author.
{\bf{ First Author$^1$, Second Author$^2$ \ and Third Author$^3$ }}
%% Here you write your institute name(s) and address(es),
%% the number in $^..$ indicates your author number, for example:
$^1$ {European Southern Observatory, Casilla 19001, Santiago 19, Chile} \\
$^2$ {Cerro Tololo Inter-American Observatory, National Optical Astronomy
Observatories, Casilla 603, La Serena, Chile} \\
$^3$ {Las Campanas Observatory, Carnegie Inst. of Washington, Casilla
601, La Serena, Chile}
%% If you use any personal Latex commands in your abstract, please include
%% their definitions here.
%% Within the following brackets you place your text:
{This is the abstract of your paper}
%% Here you write which journal accepted your paper, for example:
{ Accepted by Astron. J. }
%% Here you may write the e-mail address of one or more of the authors
%% who will act as contact person for preprint requests and
%% details of availability of the paper via the World Wide Web. For example:
{E-mail contact: rb@ast.man.ac.uk,\newline preprint available at
http://axp2.ast.man.ac.uk:8000/Preprints.html}
\end{document}
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
%%% %%%
%%% LaTeX macro for DISSERTATION ABSTRACTS %%%
%%% Please use the following macro for your thesis abstract and return %%%
%%% to rb@ast.man.ac.uk %%%
%%% %%%
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
\documentstyle{article}
\textwidth 18cm
\textheight 23cm
\oddsidemargin -1cm
\topmargin 0cm
\parskip 0.15cm
\parindent 0pt
\small
\begin{document}
\begin{center}
%% If you use any personal Latex commands in your abstract, please include
%% their definitions here.
%% Between these brackets you write the title of your thesis:
{\Large\bf{Title of Thesis}}
\vspace*{0.5cm}
%% Here comes your name
{\bf{ Author }}
%% Here you write the institute where your thesis work was conducted, e.g.:
{Thesis work conducted at: Steward Observatory, University of Arizona, USA}
%% Here comes your present postal address (if you are about to move and know
%% your coming address give it as well) e.g.:
{Current address: European Southern Observatory, Casilla 19001,
Santiago 19, Chile}
%% (if you use this part, remove %%)
%% {Address as of XX XXX 1997: }
%% Here comes your e-mail address:
{Electronic mail: doctor@sun.institute.edu}
%% Name of your adviser:
{Ph.D dissertation directed by: Galileo Galilei}
%% Month and Year of thesis:
{Ph.D degree awarded: Month Year}
\vspace*{0.8cm}
\end{center}
%% Within the following brackets you place your text:
{This is the abstract of your thesis}
\end{document}